X-Ray Thermal Coronae of Galaxies in Hot Clusters: Ubiquity of Embedded Mini-Cooling Cores

By Ming Sun, C. Jones, W. Forman, A. Vikhlinin, M. Donahue, M. Voit. 2006

133 citations recorded by the source corpus.

We present a systematic investigation of X-ray thermal coronae in 157 early-type and 22 late-type galaxies from a survey of 25 hot (kT > 3 keV), nearby (z < 0.05) clusters, based on Chandra archival data. Cool galactic coronae (kT = 0.5-1.1 keV generally) have been found to be common, >60% in LKs > 2L* galaxies. These embedded coronae in hot clusters are generally smaller, less luminous, and less massive than coronae in poor environments, demonstrating the negative effects of hot cluster environments on galactic coronae. Nevertheless, these coronae still manage to survive ICM stripping, evaporation, rapid cooling, and powerful AGN outflows, making them a rich source of information about gas stripping, microscopic transport, and feedback processes in the cluster environment. Heat conduction across the boundary of the coronae has to be suppressed by a factor of ≳100, which implies that the X-ray gas in early-type galaxies is magnetized and the magnetic field plays an important role in energy transfer. The luminous, embedded coronae, with high central density (0.1-0.4 cm-3), are miniversions of group and cluster cooling cores. As the prevalence of coronae of massive galaxies implies a long lifetime (≳several Gyr), there must be a heat source inside coronae to offset cooling. While we argue that AGN heating may not generally be the heat source, we conclude that SN heating can be enough as long as the kinetic energy of SNe can be efficiently dissipated. Diffuse thermal coronae have also been detected in at least 8 of 22 late-type galaxies in our sample. The fraction of luminous X-ray AGNs (>1041 ergs s-1) is not small (~5%) in our sample.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/56ec7e54b82acb5b9ca6d37d604c8aec38d13fe9

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Citations in the corpus

An Entropy Threshold for Strong Hα and Radio Emission in the Cores of Galaxy Clusters (2008, background): “Sun et al. (2007) extensively studied coronae and found they are like “mini-cooling cores” with low temperatures and high densities.”
CHANDRA STUDIES OF THE X-RAY GAS PROPERTIES OF GALAXY GROUPS (2008, background): “There are groups where a central corona exists (e.g., Sun et al. 2007), so naturally the temperature gradient at 5 - 20 kpc is large in these cases (e.g., A2462, A160, ESO 306-107, HCG 51 and NGC 6269).”
X-ray coronae in simulations of disc galaxy formation (2010, background): “…of X-ray measurements and upper limits from several studies (Benson et al. 2000; Strickland et al. 2004; Wang 2005; Tüllmann et al. 2006; Sun et al. 2007; Owen & Warwick 2009; Rasmussen et al. 2009) and extractedK-band luminosites from the 2MASS database and disc rotation velocities…”
REVISITING WITH CHANDRA THE SCALING RELATIONS OF THE X-RAY EMISSION COMPONENTS (BINARIES, NUCLEI, AND HOT GAS) OF EARLY-TYPE GALAXIES (2010, background): “See also Sun et al. (2007) for galaxies in clusters, Jeltema et al. (2008) for galaxies in groups, and Mulchaey & Jeltema (2010) for field galaxies.”
The colours of satellite galaxies in groups and clusters (2008, result): “The results of these simulations are in qualitative agreement with a recent Chandra X-ray survey of massive satellite galaxies in hot clusters by Sun et al. (2007), who found that most massive satellites do indeed have detectable hot haloes (see also Jeltema et al. 2008).”
Erratum: From dwarf spheroidals to cD galaxies: simulating the galaxy population in a ΛCDM cosmology (2010, background): “In the real Universe (Sun et al. 2007; Jeltema et al. 2008) and in hydrodynamic simulations, however, the hot atmosphere of massive satellite galaxies may survive for some considerable time after accretion.”
Hα Tail, Intracluster H II Regions, and Star Formation: ESO 137-001 in Abell 3627 (2007, methodology): “We have also examined allChandraand XMM- Newtondata forT >3 keV clusters at z<0.1 (62 clusters in total; for the work on a subsample at z<0.05, see Sun et al. 2007).”
INTRACLUSTER MEDIUM ENTROPY PROFILES FOR A CHANDRA ARCHIVAL SAMPLE OF GALAXY CLUSTERS (2009, background): “A2634 is a very low surface brightness cluster with the bright radio source 3C 465 at the center of an X-ray corona (Sun et al. 2007).”
Galaxy evolution in groups and clusters: star formation rates, red sequence fractions and the persistent bimodality (2011, background): “X-ray observations show direct evidence for the truncation of hot gas haloes around satellite galaxies in groups and clusters (Sun et al. 2007; Jeltema, Binder & Mulchaey 2008).”
Ram pressure stripping the hot gaseous haloes of galaxies in groups and clusters (2007, background): “…for the ram pressure stripping of galaxies in clusters has been provided by long (up to tens of kpc) tails of gas seen to be trailing behind several cluster galaxies (e.g., Sakelliou et al. 2005; Crowl et al. 2005; Vollmer et al. 2005; Sun & Vikhlinin 2005; Machacek et al. 2006; Sun et al. 2007a).”